The Chandra Deep Field North Survey. V. 1 Ms Source Catalogs

By W. N. Brandt, D. Alexander, A. Hornschemeier, G. Garmire, D. P. Schneider, A. Barger, F. E. Bauer, Patrick S. Broos, L. Cowie, L. Townsley and 6 more. 2001

288 citations recorded by the source corpus.

An extremely deep X-ray survey (≈1 Ms) of the Hubble Deep Field North (HDF-N) and its environs (≈450 arcmin2) has been performed with the Advanced CCD Imaging Spectrometer on board the Chandra X-Ray Observatory. This is one of the two deepest X-ray surveys ever performed; for point sources near the aim point, it reaches 0.5–2.0 and 2–8 keV flux limits of ≈3 × 10-17 and ≈2 × 10-16 ergs cm-2 s-1, respectively. Here we provide source catalogs, along with details of the observations, data reduction, and technical analysis. Observing conditions, such as background, were excellent for almost all of the exposure. We have detected 370 distinct point sources: 360 in the 0.5–8.0 keV band, 325 in the 0.5–2.0 keV band, 265 in the 2–8 keV band, and 145 in the 4–8 keV band. Two new Chandra sources in the HDF-N itself are reported and discussed. Source positions are accurate to within 0.″6–1.″7 (at ≈90% confidence), depending mainly on the off-axis angle. We also detect two highly significant extended X-ray sources and several other likely extended X-ray sources. We present basic number count results for sources located near the center of the field. Source densities of 7100 deg-2 (at 4.2 × 10-17 ergs cm-2 s-1) and 4200 deg-2 (at 3.8 × 10-16 ergs cm-2 s-1) are observed in the soft and hard bands, respectively.

Subfields: Astronomy and Astrophysics

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Citations in the corpus

The Extended Chandra Deep Field-South Survey: Chandra Point-Source Catalogs (2005, background): “Presently, the two deepest X-ray surveys are the 2 Ms Chandra Deep Field–North (CDF-N; Brandt et al. 2001, hereafter B01; Alexander et al. 2003, hereafter A03) and the 1 Ms Chandra Deep Field–South (CDF-S; Giacconi et al. 2002, hereafter G02).”
DEEP EXTRAGALACTIC X-RAY SURVEYS (2005, methodology): “Despite the many intensive studies of the HDF-N prior to the acquisition of the Chandra data, several new AGN were identified in the HDF-N based upon their observed X-ray emission (e.g., the three XBONGs; see Brandt et al. 2001a).”
The Chandra Deep Field-South: Optical Spectroscopy. I. (2003, methodology): “…redshift in the CDFS thus far is 3.70, while there are two confirmed and one uncertain high redshift sources in the CDFN at z ¼ 4:14 and 5.19 and z ¼ 4:42, respectively (Barger et al. 2002, 2003a; Brandt et al. 2001b), as well as one QSO at z ¼ 4:45 in the Lockman Hole (Schneider et al. 1998).”
The Resolved Fraction of the Cosmic X-Ray Background (2003, methodology): “The HDF-N consists of 12 observations for a total nominal exposure time of 978 ks.”
The Chandra Deep Field North Survey. XIV. X-Ray-detected Obscured AGNs and Starburst Galaxies in the Bright Submillimeter Source Population (2002, methodology): “Targeting X-ray sources detected in the 1 MsChandra Deep Field-North (CDF-N; Brandt et al. 2001) survey with SCUBA jiggle-map observations, Barger et al. (2001b) showed that submm counterparts can be found for faint X-ray sources.”
Chandra Deep Field South: The 1 Ms Catalog (2002, background): “Along with the Chandra Deep Field North (CDFN) (Hornschemeier et al. 2000, 2001; Brandt et al. 2001a, 2001b), the CDFS provides a unique data set in which to investigate both statistical and source-by-source properties of active galaxies over a large range of redshift and parameter space.”
The Fall of Active Galactic Nuclei and the Rise of Star-forming Galaxies: A Close Look at the Chandra Deep Field X-Ray Number Counts (2004, unknown): “These values are slightly lower than previous estimates in both the soft band, e.g., 0:70 0:20 (Mushotzky et al. 2000), 0:67 0:14 (Brandt et al. 2001a), 0:60 0:10 (Rosati et al. 2002), and 0:60þ0:02 0:03 (M03), and the hard band, e.g., 0:61 0:10 (Rosati et al. 2002), 0:63 0:05 (C02), and 0:44þ0:12…”
Optical and Infrared Properties of the 2 Ms Chandra Deep Field North X-Ray Sources (2003, background): “Barger et al. (2002) presented a similar catalog of the 370 X-ray point sources detected in the 1Ms CDF-N exposure (Brandt et al. 2001).”
High mass x-ray binaries as a star formation rate indicator in distant galaxies (2002, methodology): “We apply our results to (spatially unresolved) starburst galaxies observed by CHANDRA at redshifts up to z ∼ 1 in the Hubble Deep Field North and show that the calibration of the collective luminosity of HMXBs as a SFR indicator based on the local sample agrees well with the SFR estimates obtained f”
The HELLAS2XMM survey IV. Optical identifications and the evolution of the accretion luminosity in the Universe (2003, background): “This has to be compared with the 9 out of 38 identifications in the CDFN, SSA13 and LH samples (including 3 photometric redshift of faint optical sources in the LH sample).”
A Deep Chandra Survey of the Globular Cluster 47 Tucanae: Catalog of Point Sources (2005, unknown): “Assuming a ¼ 1:4 photon index power-law spectrum (Giacconi et al. 2001; Brandt et al. 2001) and NH ¼ 1:3 ; 1020 cm 2, 20 counts is a 0.5–2 keV flux of 1:63 ; 10 16 ergs cm 2 s 1, giving 2860 200 sources deg 2.”
The Hubble Higher z Supernova Search: Supernovae to z ≈ 1.6 and Constraints on Type Ia Progenitor Models (2004, result): “Bright residuals that were coincident with the nuclei of galaxies were also compared with known X-ray sources from the Chandra Deep Field–South and Chandra Deep Field–North 1 megasecond catalogs (Brandt et al. 2001; Giacconi et al. 2002).”
The Chandra Deep Field North Survey. XIII. 2 Ms Point-Source Catalogs (2003, background): “Great advances in this direction were made with the completion of two 1 Ms surveys: the Chandra Deep Field North (CDF-N; Brandt et al. 2001a, hereafter B01), and the Chandra Deep Field South (CDF-S; Giacconi et al. 2002, hereafter G02).”
The Ultraluminous X-Ray Source Population from the Chandra Archive of Galaxies (2004, methodology): “Also shown is a curve, N(> S) = 16(S/10−13)−1.7, representing the high-flux log(N(> S)) – log(S) results of the ASCA Large Sky Survey (Ueda et al. 1998) and Deep Sky Survey (Ogasaka et al. 1998) and the low-flux results from Brandt et al. (2001).”
A CATALOG OF X-RAY POINT SOURCES FROM TWO MEGASECONDS OF CHANDRA OBSERVATIONS OF THE GALACTIC CENTER (2008, background): “We found that almost all the duplicates could be removed by identifying sources with separations smaller than the prescription for positional uncertainties in Brandt et al. (2001): for sources offset from the center of each image by θ < 5′, the separation was cut at 0.”
AGN Host Galaxies at z ~ 0.4-1.3: Bulge-dominated and Lacking Merger-AGN Connection (2005, background): “The 1–2 Ms Chandra Deep Fields (CDF-N and CDF-S; Brandt et al. 2001; Giacconi et al. 2002), which have now resolved much of the cosmic X-ray background into moderate-luminosity AGNs at (Alexander et al. 2003; Barger et al. 2003;z ∼ 1 Szokoly et al. 2004), provide a unique AGN sample to probe these l”
Bayesian Estimation of Hardness Ratios: Modeling and Computations (2006, background): “Because these faint sources have only a few counts, hardness ratios are commonly used to study properties of their X-ray emission and absorption (e.g., Alexander et al. 2001, Brandt et al. 2001a, Brandt et al. 2001b, Giacconi et al. 2001, Silverman et al. 2005).”
The HELLAS2XMM Survey. II. Multiwavelength Observations of P3: An X-Ray-bright, Optically Inactive Galaxy (2002, background): “%) of the X–ray background emission below 8 keV have been detected byChandradeep surveys down to extremely faint fluxes S2−8keV < 10−15 erg cm−2 s−1 (Mushotzky et al. 2000; Giacconi et al. 2001; Hornschmeier et al. 2001; Brandt et al. 2001; Tozzi et al. 2001).”
A Deep Chandra Catalog of X-Ray Point Sources toward the Galactic Center (2003, methodology): “This surface density of sources is much higher than that of extragalactic sources observed in fields far from the Galactic plane (Brandt et al. 2001; Rosati et al. 2002).”
A Unified, Merger-driven Model of the Origin of Starbursts, Quasars, the Cosmic X-Ray Background, Supermassive Black Holes, and Galaxy Spheroids (2005, unknown): “This picture has been confirmed as deep surveys with ChandraandXMM-Newtonhave resolved most or all of the X-ray background into discrete sources, primarily obscured and unobscured AGN (Brandt et al. 2001; Hasinger et al. 2001; Rosati et al. 2002; Giacconi et al. 2002; Baldi et al. 2002).”